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Propagation of type II associated CME using SHEBA and solar wind properties from ACE

Created: 2014-02-11 16:26:36      Last updated: 2014-02-17 14:51:22

This workflow firstly selects the fastest CME from the wind_typeii_soho_cme catalogue of the heliophysics event catalogue (HEC). It then finds properties of this CME from soho_lasco_cme and properties of the associated flare from goes_sxr_flare. The CME and flare properties are used to run the SHEBA propagation model to find an ETA range at Earth. The average solar wind speed at this time range is then used to re-define the CME speed (this accounts for solar wind drag). The new CME speed is then used in a second run of the SHEBA propagation model to find an ETA at Earth (or any chosen destination). This workflow is based on the design of 

when_do_the_fastest_type_ii_cme_should_be_detected_throughout_all_the_heliosphere___returns_single_values__not_a_list__777405.t2flow

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Taverna 2

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Avatar Ie Eoincar

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Version History

In chronological order:

  1. Propagation of type II associated CME using SHEBA and solar wind properties from ACE

    Created by Eoincar on Tuesday 11 February 2014 16:26:31 (UTC)

  2. Propagation of type II associated CME using SHEBA and solar wind properties from ACE

    Created by Eoincar on Friday 14 February 2014 17:58:48 (UTC)

    Revision comment:

    Added inputs: Start time, end time and location at which eta is to be calculated e.g., EARTH, MARS etc.

  3. Propagation of type II associated CME using SHEBA and solar wind properties from ACE

    Created by Eoincar on Monday 17 February 2014 14:51:22 (UTC)

    Revision comment:

    This workflow firstly selects the fastest CME from the wind_typeii_soho_cme catalogue of the heliophysics event catalogue (HEC). It then finds properties of this CME from soho_lasco_cme and properties of the associated flare from goes_sxr_flare. The CME and flare properties are used to run the SHEBA propagation model to find an ETA range at Earth. The average solar wind speed at this time range is then used to re-define the CME speed (this accounts for solar wind drag). The new CME speed is then used in a second run of the SHEBA propagation model to find an ETA at Earth (or any chosen destination). This workflow is based on the design of 

    when_do_the_fastest_type_ii_cme_should_be_detected_throughout_all_the_heliosphere___returns_single

    This now has inputs of start time, end time and destination at which ETA is to be calculated

     



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Workflow Other workflows that use similar services (21)

Only the first 2 workflows that use similar services are shown. View all workflows that use these services.


Taverna 2
Uploader
2577?size=60x60 Ie David PS

Workflow When do the Fastest type II CME should be ... (2)

Thumb
The fastest CME is found from an interval of time, and propagated to Earth, in two steps, first to obtain the Solar wind speed at Earth and then propagated again with a more reasonable CME speed. The output produces Min-Max ETAs for each object in the heliosphere and the plots of the final propagation model. This Workflow was produced as one of the challenges in the HELIO CDAW-IV hosted at TCD

Created: 2012-10-21 | Last updated: 2013-03-20

Credits: User David PS User Eoincar User Gab User Baptiste Cecconi User Shanem User Jbyrne User Florian Mayer User Natasha User A lynnyk

Attributions: Workflow LASCO_CME_QUERY Workflow LASCO_CME_QUERY Workflow MDES simple execution Workflow timeToTimeRange Workflow Forward CME propagation model (SHEBA) - defined outputs Workflow When did the fastest type II CME happened? Workflow Goes Flare Check WF Workflow 100CME_task1 Workflow Extract average Solar wind speed from ACE data

Taverna 2
Uploader
3463?size=60x60 Gab

Workflow When do the Fastest type II CME should be ... (1)

Thumb
The fastest CME is found from an interval of time, and propagated to Earth, in two steps, first to obtain the Solar wind speed at Earth and then propagated again with a more reasonable CME speed. The output produces Min-Max ETAs for each object in the heliosphere and the plots of the final propagation model. This Workflow was produced as one of the challenges in the HELIO CDAW-IV hosted at TCD

Created: 2013-03-21

Credits: User Gab User Anja Le Blanc User David PS

Attributions: Workflow When did the fastest type II CME happened?

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